The online star radiation simulations on this page will help us to understand what star radiation is like and to learn about the important physical concept of the blackbody and the Planck’s Law.
What is star radiation
Radiation is a physical phenomenon that refers to the emission and propagation of energy in the form of electromagnetic waves or subatomic particles. It can be natural or artificial and has various applications and effects in different contexts. Star radiation is the light and energy emitted by stars due to nuclear fusion processes in their nuclei, which transform light elements, such as hydrogen, into heavier elements, releasing energy in the form of electromagnetic radiation. This radiation covers a wide range of the spectrum, from infrared and visible light to ultraviolet and, in some cases, X-rays and gamma rays, depending on the temperature and type of star.
Microwave background radiation
Star radiation should not be confused with microwave background radiation. Microwave background radiation is homogeneous microwave radiation that permeates the entire universe, being the remnant of the Big Bang. Although both star radiation and microwave background radiation are forms of radiation, star radiation is emitted continuously by present-day stars, while microwave background radiation is a relic of the early universe, observable in the microwave region and virtually unchanging in time.
Blackbody radiation. Planck’s Law
A blackbody is a theoretical object that absorbs all radiation incident on it and emits radiation continuously as a function of its temperature. The radiation emitted by a black body is called black body radiation and its value is established by Planck’s Law.
Stars behave very much like a black body, absorbing the radiation that reaches their surface and emitting radiation in the form of light and heat. The temperature of a star determines the spectrum of radiation it emits. Wien’s displacement law states that the hotter a star is, the shorter the dominant wavelengths in its radiation spectrum. Therefore, hot stars emit a greater proportion of radiation in the ultraviolet and visible wavelength range. Cooler stars emit a greater proportion of radiation in the infrared wavelength range.
In addition to temperature, star radiation also depends on the composition of the stars. The constituent elements affect the absorption and emission of radiation at specific wavelengths, resulting in different radiation spectra. The study of these spectral lines allows astronomers to determine the chemical composition of stars and to obtain information about their temperature and other characteristics.
Star radiation simulations
Blackbody
How does the blackbody spectrum of the Sun work compared to visible light? Learn about the blackbody spectrum of the sun, a light bulb, a furnace, and the earth. Adjust the temperature to see the wavelength and intensity of the spectrum changes. See the color of the peak of the spectral curve and observe in a practical way the operation of Planck’s Law..
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Star radiation
The color of a star depends on its surface temperature and can be red, yellow, white, or blue. The higher the temperature, the bluer the star; the lower the temperature, the redder the star. Therefore, by observing the color of the star, its temperature can be deduced.
Equilibrium of radiation on Earth
This animation summarizes the various factors involved in the Earth’s radiation balance.
The History of Ancient Environments, Climate, and Life
Introduction to Deep Earth Science
Sensing Planet Earth – Water and Ice
Sensing Planet Earth – From Core to Outer Space
The Radio Sky II: Observational Radio Astronomy
The Radio Sky I: Science and Observations
Our Place in the Universe
